HAL : in2p3-00291652, version 1

arXiv : 0804.4367

DOI : 10.1111/j.1365-2966.2008.13393.x

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Monthly Notices of the Royal Astronomical Society 388 (2008) 347-356

The complex light-curve of the afterglow of GRB071010A

S. Covino, P. D'Avanzo, A. Klotz 1, 2, D. A. Perley, L. Amati, S. Campana, G. Chincarini, A. Cucchiara, V. D'Elia, D. Guetta, C. Guidorzi, D. A. Kann, A. Küpcü Yolda?, K. Misra, G. Olofsson, G. Tagliaferri, L. A. Antonelli, E. Berger, J. S. Bloom, M. Böer 2, C. Clemens, F. D'Alessio, M. Della Valle, S. Di Serego Alighieri, A. V. Filippenko, R. J. Foley, D. B. Fox, D. Fugazza, J. Fynbo, B. Gendre 3, P. Goldoni 4, 5, 6, J. Greiner, D. Kocevksi, E. Maiorano, N. Masetti, E. Meurs, M. Modjaz, E. Molinari, A. Moretti, E. Palazzi, S. B. Pandey, S. Piranomonte, D. Poznanski, N. Primak, P. Romano, E. Rossi, R. Roy, J. M. Silverman, L. Stella, G. Stratta, V. Testa, S. D. Vergani, F. Vitali, F. Zerbi

(06/2008)

We present and discuss the results of an extensive observational campaign devoted to GRB071010A, a long-duration gamma-ray burst detected by the Swift satellite. This event was followed for almost a month in the optical/near-infrared (NIR) with various telescopes starting from about 2min after the high-energy event. Swift-XRT observations started only later at about 0.4d. The light-curve evolution allows us to single out an initial rising phase with a maximum at about 7min, possibly the afterglow onset in the context of the standard fireball model, which is then followed by a smooth decay interrupted by a sharp rebrightening at about 0.6d. The rebrightening was visible in both the optical/NIR and X-rays and can be interpreted as an episode of discrete energy injection, although various alternatives are possible. A steepening of the afterglow light curve is recorded at about 1d. The entire evolution of the optical/NIR afterglow is consistent with being achromatic. This could be one of the few identified GRB afterglows with an achromatic break in the X-ray through the optical/NIR bands. Polarimetry was also obtained at about 1d, just after the rebrightening and almost coincident with the steepening. This provided a fairly tight upper limit of 0.9% for the polarized-flux fraction.

1 :	Centre d'étude spatiale des rayonnements (CESR)
	CNRS : UMR5187 – Observatoire Midi-Pyrénées – INSU – Université Paul Sabatier [UPS] - Toulouse III
2 :	Observatoire de Haute-Provence (OHP)
	CNRS : USR2207 – INSU – Université de Provence - Aix-Marseille I
3 :	Laboratoire d'Astrophysique de Marseille (LAM)
	CNRS : UMR6110 – INSU – Université de Provence - Aix-Marseille I
4 :	Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA)
	CEA : DSM/DAPNIA
5 :	AstroParticule et Cosmologie (APC)
	CNRS : UMR7164 – IN2P3 – Observatoire de Paris – Université Paris VII - Paris Diderot – CEA : DSM/IRFU
6 :	Service d'Astrophysique (SAp)
	CEA : DSM/IRFU

équipe(s) de recherche : APC - AHE

Thème(s)

:

Physique/Astrophysique/Cosmologie et astrophysique extra-galactique Planète et Univers/Astrophysique/Cosmologie et astrophysique extra-galactique Planète et Univers/Astrophysique

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Contributeur : Simone Lantz <>

Soumis le : Lundi 30 Juin 2008, 09:55:14

Dernière modification le : Vendredi 22 Juin 2012, 21:35:02